Tsunamis in Galaxy Clusters: Heating of Cool Cores by Acoustic Waves

Fujita, Yutaka; Suzuki, Takeru; Wada, Keiichi

doi:10.1086/380113

Cited by 26 publications

(32 citation statements)

References 75 publications

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“…Since the velocity amplitude is relatively large, the waves steepen and become weak shocks as shown in one-dimensional simulations (Fujita et al 2004b). Because of the pressure coming from the momentum of the waves, the coolest and densest gas noticeably shifts from the cluster center at Gyr, and the shift is clearly seen at t տ 0.7 Gyr (Fig.…”

Section: Resultsmentioning

confidence: 92%

Strong Turbulence in the Cool Cores of Galaxy Clusters: Can Tsunamis Solve the Cooling Flow Problem?

Fujita

Matsumoto

Wada

2004

ApJ

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On the basis of high-resolution two-dimensional hydrodynamic simulations, we show that the bulk gas motions in a cluster of galaxies, which are naturally expected during the process of the hierarchical structure formation of the universe, have a serious impact on the core. We found that the bulk gas motions represented by acousticgravity waves create local but strong turbulence, which reproduces the complicated X-ray structures recently observed in cluster cores. Moreover, if the wave amplitude is large enough, they can suppress the radiative cooling of the cores. Contrary to the previous studies, the heating is operated by the turbulence, not weak shocks. The turbulence could be detected in near-future space X-ray missions such as Astro-E2.

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Section: Resultsmentioning

confidence: 92%

Strong Turbulence in the Cool Cores of Galaxy Clusters: Can Tsunamis Solve the Cooling Flow Problem?

Fujita

Matsumoto

Wada

2004

ApJ

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“…Ruszkowski & Begelman 2002;Zakamska & Narayan 2003;Voigt & Fabian 2004;Conroy & Ostriker 2008;Bogdanović et al 2009;Ruszkowski & Oh 2010, 2011 and stirring by the motions of substructures (Fujita et al 2004;Ruszkowski & Oh 2011). However, the principle energy source is expected to be feedback from an accreting supermassive black hole (SMBH).…”

Section: Introductionmentioning

confidence: 99%

AGN jet feedback on a moving mesh: cocoon inflation, gas flows and turbulence

Bourne¹,

Sijacki

2017

Monthly Notices of the Royal Astronomical Society

101

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In many observed galaxy clusters, jets launched by the accretion process on to supermassive black holes, inflate large-scale cavities filled with energetic, relativistic plasma. This process is thought to be responsible for regulating cooling losses, thus moderating the inflow of gas on to the central galaxy, quenching further star formation and maintaining the galaxy in a red and dead state. In this paper, we implement a new jet feedback scheme into the moving mesh-code arepo, contrast different jet injection techniques and demonstrate the validity of our implementation by comparing against simple analytical models. We find that jets can significantly affect the intracluster medium (ICM), offset the overcooling through a number of heating mechanisms, as well as drive turbulence, albeit within the jet lobes only. Jet-driven turbulence is, however, a largely ineffective heating source and is unlikely to dominate the ICM heating budget even if the jet lobes efficiently fill the cooling region, as it contains at most only a few percent of the total injected energy. We instead show that the ICM gas motions, generated by orbiting substructures, while inefficient at heating the ICM, drive large-scale turbulence and when combined with jet feedback, result in line-ofsight velocities and velocity dispersions consistent with the Hitomi observations of the Perseus cluster.

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“…In particular, hydrodynamical simulations of merging clusters have shown that moving substructures can generate turbulence in the ICM by means of shearing instabilities (Roettiger et al 1997;Norman & Bryan 1999a;Takizawa 2000;Ricker & Sarazin 2001;Fujita et al 2004a;Takizawa 2005;Dolag et al 2005;Iapichino & Niemeyer 2008;Vazza et al 2009;Planelles & Quilis 2009).…”

Section: Introductionmentioning

confidence: 99%

The impact of numerical viscosity in SPH simulations of galaxy clusters

Valdarnini

2011

A&A

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The goal of this paper is to investigate in N-body/SPH hydrodynamical cluster simulations the impact of artificial viscosity on the ICM thermal and velocity field statistical properties. To properly reduce the effects of artificial viscosity, a time-dependent artificial viscosity scheme is implemented in an SPH code in which each particle has its own viscosity parameter, whose time evolution is governed by the local shock conditions. The new SPH code is verified in a number of test problems with known analytical or numerical reference solutions and is then used to construct a large set of N-body/SPH hydrodynamical cluster simulations. These simulations are designed to study in SPH simulations the impact of artificial viscosity on the thermodynamics of the ICM and its velocity field statistical properties by comparing results extracted at the present epoch from runs with different artificial viscosity parameters, cluster dynamical states, numerical resolution, and physical modeling of the gas. Spectral properties of the gas velocity field are investigated by measuring the velocity power spectrum E(k) for the simulated clusters. Over a limited range, the longitudinal component E c (k) exhibits a Kolgomorov-like scaling ∝k −5/3 , whilst the solenoidal power spectrum component E s (k) is strongly influenced by numerical resolution effects. The dependence of the spectra E(k) on dissipative effects is found to be significant at length scales < ∼ 100−300 kpc, with viscous damping of the velocities being less pronounced in the runs with the lowest artificial viscosity. The turbulent energy density radial profile E turb (r) is strongly affected by the numerical viscosity scheme adopted in the simulations, with the turbulent-to-total energy density ratios being higher in the runs with the lowest artificial viscosity settings and lying in the range between a few percent and ∼10%. These values are in accord with the corresponding ratios extracted from previous cluster simulations based on mesh-based codes. The radial entropy profiles show a weak dependence on the artificial viscosity parameters of the simulations, with a small amount of entropy mixing being present in cluster cores. At large cluster radii, the mass correction terms to the hydrostatic equilibrium equation are affected little by the numerical viscosity of the simulations, indicating that the X-ray mass bias is already accurately estimated in standard SPH simulations. The results presented here indicate that in individual SPH cluster simulations at least N > ∼ 256 3 gas particles are necessary to provide a correct description of turbulent spectral properties over a decade in wavenumbers, whilst radial profiles of thermodynamic variables can be reliably obtained using N > ∼ 64 3 particles. Finally, simulations in which the gas can cool radiatively are characterized by the presence in the cluster inner regions of high levels of turbulence, generated by the interaction of the compact cool gas core with the ambient medium. These findings strongly support t...

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Tsunamis in Galaxy Clusters: Heating of Cool Cores by Acoustic Waves

Cited by 26 publications

References 75 publications

Strong Turbulence in the Cool Cores of Galaxy Clusters: Can Tsunamis Solve the Cooling Flow Problem?

Strong Turbulence in the Cool Cores of Galaxy Clusters: Can Tsunamis Solve the Cooling Flow Problem?

AGN jet feedback on a moving mesh: cocoon inflation, gas flows and turbulence

The impact of numerical viscosity in SPH simulations of galaxy clusters

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